We plot in Fig.(REF ) left panel, the ejected mass as a function of gravitational masses \(M_1, M_2\)  for \(M_i \in [1.2,1.6]\)  in our analysis with the DD2 EoS. As a rule of thumb we see that smaller mass ratio \(q\equiv M_</M_>\)  provide larger \(M_{ej}\) . The experimental measurement of the KN peak bolometric luminosity and spectral time series usually depend on the conditions of transparency after the ejection of matter parameterized through the opacity, \(\kappa \) . For early emission, typically \(\kappa \sim {0.1 \mathrm {~cm}^{2} \mathrm {~g}^{-1}}\)  while for later r-powered emission \(\kappa \)  could be a factor of 10 or more larger. The peak values and are given [1]} by \(t_{{peak}}=4.9 \mathrm {~d} \times \left(\frac{M_{ej}}{10^{-2} M_{\odot }}\right)^{\frac{1}{2}}\left(\frac{\kappa }{10 \mathrm {~cm}^{2} \mathrm {~g}^{-1}}\right)^{\frac{1}{2}}\left(\frac{v_{\mathrm {ej}}}{0.1}\right)^{-\frac{1}{2}}\)  .
For a BNS the measurable magnitudes can be fitted to the Black Body power spectrum [2]} and from GW170817 some constraints appear for masses i.e. total mass \(M \approx 2.74 M_{\odot }\) , and individual masses of \(M_{1} \approx (1.36-1.6) M_{\odot }\)  and \(M_{2} \approx (1.17-1.36) M_{\odot }\) . Also from this analysis marginalized over the selection methods, it was obtained that the radius of the progenitors \(R_{1} \sim (10.8-11.9) \pm 2 \mathrm {~km}\)  and \(R_{2} \sim (10.7-11.9) \pm 2 \mathrm {~km}\)  and the tidal deformability parameters \(\Lambda _{1}<\Lambda _{2}, \Lambda _{1}<500\)  and \(\Lambda _{1}<1000\) . Under this additional input they find \(\tilde{\Lambda }(310-345)_{-245}^{+691}\)  and \(R_{1.4}=8.7-14.1 \mathrm {~km},\)  where the binary tidal deformability \(\tilde{\Lambda }\)  is defined as \(\tilde{\Lambda } \equiv \frac{16}{13}\left[\frac{\Lambda _{1} M_{1}^{4}\left(M_{1}+12 M_{2}\right)}{\left(M_{1}+M_{2}\right)^{5}}+1 \leftrightarrow 2\right]\)  which is most precisely derived.
